ISRN High Energy Physics

Volume 2013 (2013), Article ID 713508, 9 pages

http://dx.doi.org/10.1155/2013/713508

## Gravity with Extra Dimensions and Dark Matter Interpretation: A Straightforward Approach

^{1}Universidade Federal do Paraná (UFPR), Campus Palotina, 85950-000 Palotina, PR, Brazil^{2}Centro de Matemática, Computação e Cognição, Universidade Federal do ABC, 09210-170 Santo André, SP, Brazil

Received 8 May 2013; Accepted 6 June 2013

Academic Editors: G. A. Alves, G. Bonvicini, C. A. D. S. Pires, and A. Koshelev

Copyright © 2013 C. H. Coimbra Araújo and Roldão da Rocha. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

#### Abstract

Any connection between dark matter and extra dimensions can be cognizably
evinced from the associated effective energy-momentum tensor. In order to investigate and
test such relationship, a higher dimensional spacetime endowed with a factorizable general
metric is regarded to derive a general expression for the stress tensor—from the Einstein-Hilbert action—and to elicit the effective gravitational potential. A particular construction
for the case of six dimensions is provided, and it is forthwith revealed that the missing
mass phenomenon may be explained, irrespective of the dark matter existence. Moreover,
the existence of extra dimensions in the universe accrues the possibility of a straightforward
mechanism for such explanation. A configuration whose density profile coincides with the
Newtonian potential for spiral galaxies is constructed, from a 4-dimensional isotropic metric
plus extradimensional components. A Miyamoto-Nagai *ansatz* is used to solve Einstein equations.
The stable rotation curves associated with such system are computed, in full compliance
with the observational data, without fitting techniques. The density profiles are reconstructed
and compared to the ones obtained from the Newtonian potential.

#### 1. Introduction

General relativity (GR) provides solutions to the Einstein equations that currently offer important support to understand, for instance, black holes and cosmology. Mainly in the last two decades, such formalism was extended for extradimensional spacetimes. There are many motivations to consider such approach: from the Kaluza-Klein—and string theory as well—idea of unified fields to the recent effort to deal with the hierarchy problem from the idea of diluting gravity in submillimetric extra dimensions [1, 2]. Another motivation—indeed more fundamental for GR—is that higher dimensions may play a fundamental role to unravel profound interpretations concerning the nature of spacetime. On this behalf, a series of works deal with a -dimensional metric splitting, in order to find solutions for the Einstein equations, in both static or stationary spherical/axisymmetric geometries. The static, spherically symmetric solutions of Kaluza-Klein theory were calculated independently by several authors [3]. For instance, in [4, 5] some stationary spherically symmetric solutions on Kaluza-Klein theory are provided, as well as on 5-dimensional GR [6]. Furthermore, in [7] some asymptotically flat Kaluza-Klein solutions, corresponding to regular black holes in four dimensions, are regarded, and prominent features concerning thermal evaporation are presented. Such formalism is generalized in a -dimensional scenario [8]. It is accomplished in the so-called abelian Kaluza-Klein theory—possessing the as its internal isometry group—whose lower dimensional case was investigated in [9, 10]. The rotating dyonic black holes of Kaluza-Klein theory were investigated [11] withal, and the explicit connection between such models and extradimensional theories is explored in [12–14].

Therewith, one of the most outstanding noncompact extra dimensions usages is the Randall-Sundrum (RSI) model, wherein the so-called braneworld is embedded in an space [1, 2]. Moreover, some large extra dimensions formalisms were investigated in a ()-dimensional setting. The Einstein equations with negative bulk cosmological constant and a 3-brane, with appropriately tuned energy-momentum tensor, were solved [15–17]. In the case of two extra dimensions, which will be considered as a particular case of our formalism, some aspects were approached in [18].

The pivotal physical motivation in our formulation is that gravity with extra dimensions can possibly shed new light on the so-called “dark matter” puzzle [19–24]. The idea is not a novelty since some theories, as universal extra dimensions [25], and some variants of Kaluza-Klein theories as well present particles corresponding to extradimensional excitation modes, representing a dark matter candidate (for a review see [26]). Here the approach is different, in the sense that it is argued whether the existence of higher dimensional spacetimes suffices to explain the missing mass problem (*aka* “dark matter”), without any specific dark particle.

In order to precisely ascertain what this assumption infuses in the dark matter problem, we delve into a generalization where our universe has dimensions. Moreover, at a first glance nothing precludes the matter to live—or leak as well—in the extra dimensions (see, e.g., at the level of particle physics, the UED proposition [25]). In what follows the formalism is developed *a la* Kaluza-Klein.

Accordingly from such scenario, an Einstein–Hilbert gravitational action where denotes the matter Lagrangian, leads to the field equations where and denotes the extra dimensions. Hereon the tensor components and are, respectively, denoted by and (the same for the curvature tensor and scalar and for the metric components as well). No modification is considered for the gravitational constant .

Given such approach, in Section 2 the spacetime metric is split, in order to express the 4-dimensional stress tensor. It infuses some interpretations about the extra terms, appearing due to the inclusion of new dimensions (Section 3). In Section 4 the equations of motion are developed, and in Section 5 we calculate—by linearized gravity—the Newtonian limit and a modified Poisson equation for the theory. Section 6 is dedicated to show how one can interpret dark matter as a prominent pure effect, coming from the spacetime extra dimensions. We provide particular cases where two extra dimensions are regarded. Stable galaxy rotation curves are presented together with their associated analytical expression when the system is axisymmetric in Section 7. Finally in Section 8 some results with real galaxies are presented and analyzed which, together with the results in Section 7, put our formalism in compliance with observational data.

A companion paper shows a phenomenological example [20], as well as other semiphenomenological ones provided by [19]. The assumptions here are straightforward, and quantum field theory is not explicitly taken into account. GR is the theoretical limit concerning the present work. In this paper, unless explicitly mentioned, , and the signature adopted for the -dimensional part of the metric is . In addition, it is considered *ab initio* that the extradimensional part is constituted by spacelike coordinates.

#### 2. Splitting the Metric

Our universe is supposed to have dimensions. Initially, the extra dimensions compactification is kept apart. The most general metric for such universe is given by where and . Furthermore we consider the convention to make the metric as a function of coordinates only: . These metric components contain the universe metric terms and the extra dimensional terms , as well as the crossed components. Equation (3) can be rewritten for convenience as where are the Kronecker symbols. The derivatives for such metric components are given by The case is considered here, motivated by formalisms, where , namely, Randall-Sundrum warped metrics [1, 2] and other physically relevant cases [12–14, 21–23, 27–40]. In particular, a comprehensive program on observation and measurements on braneworld effects in astrophysics and particle physics is provided in [35, 36]. Furthermore, some generalizations regarding variable tension braneworld models and cognizable physical effects were presented [37–40].

The inverse metric is written as
and the derivatives are straightforwardly provided by (5):
Assuming that the spacetime has a connection presenting *no* torsion, one yields the following Christoffel symbols: . Splitting this last expression by (6) and (7) it reads
The Ricci tensor components are well known to be written as
Taking into account that the terms of the metric depend solely on , the equation above reads
The splitting (6) and the derivatives (7) of the metric in the Christoffel symbols (8) lead to the following expressions for (10):
where is the conventional () Ricci tensor.

#### 3. The Energy-Momentum Tensor

Consider now the Einstein tensor components , where is the scalar curvature. For a stress tensor written as , one can follow the same arguments accomplished for . Introducing the results obtained in the previous Section in (2), the split components of the stress tensor are given by The tensor represents the energy/pressure content in the -dimensional landscape. This is the part that is clearly of paramount interest. Regardless of , here it is assumed that only the visible part can bring some light to observational issues. From the expression developed for , (11), the influence of extra dimensions is evident. From (11), (12), and (13) it yields where represents the -dimensional influence and denotes the correction elicited uniquely from extra dimensions where explicitly Note that the stress has the conventional form for the Einstein tensor . The tensor represents a “curvature” term evinced from the presence of extra dimensions, and is given by In addition, from the action (1) the stress tensor can be derived from the conventional definition . In this new approach, it is clear that the -dimensional part is proportional to the Lagrangian multiplied by and some quantity from the variation .

#### 4. An Expression for the Equations of Motion

A general Lagrangian for the gravitating test particles in a spacetime with extra dimensions, with metric elements , can be written as where . The motion equations come from the Euler-Lagrange expression . As and , it follows that and . It immediately yields Likewise, the term can be developed: Now Since are cyclic variables, it reads the integration constant a constant vector. Hence . Inserting the terms together, multiplying by , and using (22), the equations of motion are derived: Clearly it is possible to realize that the extra dimensions induce an external force in the system that depends on and .

#### 5. Equation for the Visible Field

The main aim now is to compute the gravitational potential in the Newtonian limit since galaxies and clusters can be described physically as Newtonian objects, corresponding to the approximation in which gravity is weak. The weak limit is assumed uniquely in the 4-dimensional spacetime: the deviation of the 4-dimensional metric is small ( denotes the Minkowski metric). For the linearized gravity, the stress (15) is essentially written from linearized curvature as where is the traceless part of and . Linearized gravity has a gauge freedom given by , where denotes the Lie derivative with respect to the generators of a differential diffeomorphism. To the first order, such transformation represents the same physical transformation as . This gauge freedom is used to simplify the linearized Einstein equation. Solving the equation for , a gauge transformation [41] that leads to —similar to the Lorentz gauge condition—can be elicited to obtain the simplified Einstein equation For the extra part it reads When gravity is weak, the linear approximation to GR should be valid. There exists a global inertial coordinate system of such that where is the time direction associated with this coordinate system. This equation can be interpreted as the modified Poisson equation considering a universe with more than dimensions.

#### 6. Extra Dimensions and the Interpretation of Dark Matter

Define , where is a 3-space scalar field. Furthermore consider a line element , where is the world line for the extra sector, denotes the extra coordinates, and are potentials associated to extra dimensions.

If one asserts, as a first approximation, that (i.e., *not* similar to impose vacuum in the extra space, since now becomes ), (12) implies at first order the sigma model for the extra part, where denotes the diagonal matrix representing the metric associated with the system, which implies
yielding the following equation:
or in other words
It means that our visible matter density profile is provided uniquely by the 4-dimensional field. If extra dimensions have some impact on the theory, certainly it is not as extra matter, but it appears at least as the term in (29). In matter models applicable to a galactic context pressure arises from the velocity dispersion in the motion of particles or from exchange of momentum among particles through collisions, ionized interstellar baryonic gases. An extra pressure for the same energy density could be possible for the star gases, which have no equation of state but would introduce modifications on the equation of state of the interstellar gases. Instead, the extra term in (29) has the form of a tidal force produced by the purely geometric effect of the extra dimensions. Likewise, the equation of motion does not necessarily dismiss the influence of the extra field, as it can be illustrated by the following example. A general metric can be written for the simplified case of six dimensions as [19], where is the -dimensional line element. Now, in the Newtonian limit the motion is conceived to be much slower than the speed of light, can be assumed to be in (23), and the affine parameter may be approximated by the coordinate time . Thus it follows that
As time derivatives of and are neglected, (31) leads to
that is, the equation of motion of test bodies gravitating in an orbit in a given background for our system with an effective gravitational potential . To find a form for those potentials, from (28) and (30) it yields
Nonlinear terms do not appear since the matrix is diagonal. In particular, (34) can be rewritten as
where the identification is accomplished and hence (33) has the form
Together with (35) and (36), it represents a complete system of equations for a gravitational effective potential in 4-dimensions, assuming a 6-dimensional universe. Note as well that (36) is the Laplace equation in flat 3-dimensional space, and therefore can be taken as a solution of Laplace equation for an appropriate Newtonian source of any symmetry. The form of can be indeed expressed as the point source potential ~1/ for a Newtonian system.

In a system whose acceleration , (32), has radial direction, for example, an idealized system similar to a galaxy, the rotation curves for a potential are provided by

#### 7. Solutions

Now we look for a way to implement an exact Newtonian solution for the Poisson equation (35), as well as for the Laplace equation (36). As a system similar to a galaxy is regarded, the Poisson equation can be implemented, for example, by a Miyamoto-Nagai potential, and for the case of Laplace equation a Chazy-Curzon solution can be used for an axisymmetric configuration. Namely, the Miyamoto-Nagai *ansatz* is written as [42]
where , are positive constants. The Chazy-Curzon solution for a particle of mass in the position is given by [43, 44]
where . In this last, it is possible to fix and to introduce the cut method to generate a disk solution [45], such that , where is the cut parameter. Fixing values for , , and in such a way that , providing a similar light distribution of a disk galaxy [45], and (by stability issues and to prevent relativistic disks [19]) it is possible to find the set of curves given in Figure 1(a).

The stability of this last configuration is guaranteed by the positive epicyclic Newtonian parameter , as shown in Figure 1(b).

A more useful manner to analyze the effective potential is writing it as where and are constants to be determined. This is the correspondent Newtonian potential in the present formalism. Clearly, from (33) those constants are related to and as Given the present results, one can ask about the nature of the potential (41). The term comes exclusively from extra dimensions and it may be related to a “dark matter” potential as showing that our approach is equivalent to a dark matter effect, although the concept above is completely apart from the concept of extra matter.

#### 8. Probing Results with Real Galaxies

Taking into account only the stable curves, we compare in Figures 2 and 3 some optically observed rotation curves of spiral galaxies.

Here we are not providing a composition of halo dark matter velocities plus the disk gas and the velocities of stars. What is happening is that the clean stable calculated curves are simply fitting the region of interest. The unsurprising *ad hoc* adjustment of and actually could assert nothing about the astrophysical role of the extra dimensions in the model. However, the calculation of stable configurations brings realizable values for and , which makes it possible to visualize a minimum representation of a real disk galaxy. We furthermore compared our results to some phenomenological models used in astrophysics, as for instance in Navarro, Frenk & White [46]. Our model is successful when compared to the observational data [47–51].

Note that our results reproduce with great fidelity the shape of nonplanar curves, as that appearing in Figure 3(b) (data taken from [52, 53]).

#### 9. Concluding Remarks

At the present work we showed how to calculate a “dark” potential from extradimensional imprints. If extra dimensions have some impact on the theory, certainly it is not as extra matter, but it appears at least as tidal force produced by the purely geometric effect of the extra dimensions, namely, the term in (29). This is confirmed by the extra force appearing in the equations of motion.

The Newtonian limit is calculated and we accomplished the visible potential that has two main components: a term from 4-dimensional metric and another term coming exclusively from extradimensional effects. The 4-dimensional term obeys the Poisson equation, and the extra term is solved from a Laplace equation. Two situations are provided: a first approximated model and a second that arises from exact solutions of Laplace and Poisson equations, respectively, the Chazy-Curzon disk solution and Miyamoto-Nagai *ansatz*. Those examples are calculated for a case where two extra dimensions are taken into account. Moreover, any decomposition for the weak field potential hold for this formalism, with the appropriate symmetry. For instance, as the effective models for elliptic galaxies or globular clusters, in which is may be a different potential.

The extra field arises naturally from metric extra terms, and the modification of gravity shown from the calculation of rotation curves can present an explanation about the missing mass effect in astronomy. The effective potential calculated here is a source to explain the phenomenological results found in [19, 20]. The extra part of this effective potential has the form . The gradient of such potential represents the extra force associated with the presence of extra dimensions. It modifies the rotation curve profiles and rise anomalies in potential associated to clusters. The Laplacian corresponds to a “dark” density profile that is negligible compared to the visible density (see Section 6). Furthermore, the extradimensional proposal is consistent with a more general length scale and galactic morphology.

The present calculation is an alternative approach to understand the dark matter problem. In fact, to solve the dark matter problem means to solve a long list of cosmological anomalies. In this aspect, as a complement, considerations about cluster lensing are also addressed in [21–23].

#### Acknowledgments

The authors are extremely grateful to Patricio S. Letelier (*in memoriam*) for the important and profound contribution concerning interpretation and discussion of the present results. The work of C. H. Coimbra-Araújo is supported by Fundação Araucária and PDEE/CAPES Programme under Grant no. 3874-07-9. R. da Rocha is grateful to CNPq 472903/2008-0 and 304862/2009-6 for financial support.

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